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dc.date.accessioned | 2021-09-17T13:01:57Z | |
dc.date.available | 2021-09-17T13:01:57Z | |
dc.date.issued | 2021 | |
dc.identifier.uri | http://sedici.unlp.edu.ar/handle/10915/125050 | |
dc.description.abstract | The formation and stability of collisionless self-gravitating systems is a long standing problem, which dates back to the work of D. Lynden-Bell on violent relaxation, and extends to the issue of virialization of dark matter (DM) halos. An important prediction of such a relaxation process is that spherical equilibrium states can be described by a Fermi-Dirac phase-space distribution, when the extremization of a coarse-grained entropy is reached. In the case of DM fermions, the most general solution develops a degenerate compact core surrounded by a diluted halo. As shown recently, the latter is able to explain the galaxy rotation curves while the DM core can mimic the central black hole. A yet open problem is whether this kind of astrophysical core-halo configurations can form at all, and if they remain stable within cosmological timescales. We assess these issues by performing a thermodynamic stability analysis in the microcanonical ensemble for solutions with given particle number at halo virialization in a cosmological framework. For the first time we demonstrate that the above core-halo DM profiles are stable (i.e. maxima of entropy) and extremely long lived. We find the existence of a critical point at the onset of instability of the core-halo solutions, where the fermion-core collapses towards a supermassive black hole. For particle masses in the keV range, the core-collapse can only occur for Mvir≳109M⊙ starting at zvir ≈ 10 in the given cosmological framework. Our results prove that DM halos with a core-halo morphology are a very plausible outcome within nonlinear stages of structure formation. | en |
dc.format.extent | 4227-4246 | es |
dc.language | en | es |
dc.subject | Methods: numerical | es |
dc.subject | Galaxies: haloes | es |
dc.subject | Galaxies: nuclei | es |
dc.subject | Galaxies: formation | es |
dc.subject | Galaxies: structure | es |
dc.subject | Dark matter | es |
dc.title | On the formation and stability of fermionic dark matter haloes in a cosmological framework | en |
dc.type | Articulo | es |
sedici.identifier.other | arXiv:2012.11709 | es |
sedici.identifier.other | doi:10.1093/mnras/staa3986 | es |
sedici.identifier.issn | 0035-8711 | es |
sedici.identifier.issn | 1365-2966 | es |
sedici.creator.person | Argüelles, Carlos Raúl | es |
sedici.creator.person | Díaz, Manuel | es |
sedici.creator.person | Krut, Andreas | es |
sedici.creator.person | Yunis, Rafael | es |
sedici.subject.materias | Ciencias Astronómicas | es |
sedici.description.fulltext | true | es |
mods.originInfo.place | Facultad de Ciencias Astronómicas y Geofísicas | es |
sedici.subtype | Articulo | es |
sedici.rights.license | Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) | |
sedici.rights.uri | http://creativecommons.org/licenses/by-nc-sa/4.0/ | |
sedici.description.peerReview | peer-review | es |
sedici.relation.journalTitle | Monthly Notices of the Royal Astronomical Society | es |
sedici.relation.journalVolumeAndIssue | vol. 502, no. 3 | es |